TESS Hunt for Young and Maturing Exoplanets (THYME) III: a two-planet system in the 400 Myr Ursa Major Group

Mann, Andrew W.; Johnson, Marshall C.; Vanderburg, Andrew; Kraus, Adam L.; Rizzuto, Aaron C.; Wood, Mackenna L.; Bush, Jonathan L.; Rockcliffe, Keighley; Newton, Elisabeth R.; Latham, David W.; Mamajek, Eric E.; Zhou, George; Quinn, Samuel N.; Thao, Pa Chia; Benatti, Serena; Cosentino, Rosario; Desidera, Silvano; Harutyunyan, Avet; Lovis, Christophe; Mortier, Annelies; Pepe, Francesco A.; Poretti, Ennio; Wilson, Thomas G.; Kristiansen, Martti H.; Gagliano, Robert; Jacobs, Thomas; LaCourse, Daryll M.; Omohundro, Mark; Schwengeler, Hans Martin; Terentev, Ivan A.; Kane, Stephen R.; Hill, Michelle L.; Rabus, Markus; Esquerdo, Gilbert A.; Berlind, Perry; Collins, Karen A.; Murawski, Gabriel; Sallam, Nezar Hazam; Aitken, Michael M.; Massey, Bob; Ricker, George R.; Vanderspek, Roland; Seager, Sara; Winn, Joshua N.; Jenkins, Jon M.; Barclay, Thomas; Caldwell, Douglas A.; Dragomir, Diana; Doty, John P.; Glidden, Ana; Tenenbaum, Peter; Torres, Guillermo; Twicken, Joseph D.; Villanueva, Steven

doi:10.48550/arxiv.2005.00047

Cited by 10 publications

(13 citation statements)

References 119 publications

(144 reference statements)

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“…This means that the formation and migration of the planets of the AU Mic system occurred within the disk. AU Mic b is the third young (< 100My) small planet with a published measurement of its spin-orbit alignment, after DS Tuc b (Zhou et al 2020) and HD 63433 b (Mann et al 2020). Noticeably, all three planets show prograde and aligned orbits.…”

Section: Discussionmentioning

confidence: 85%

Transmission spectroscopy and Rossiter-McLaughlin measurements of the young Neptune orbiting AU Mic

Πάλλη

Oshagh

Casasayas-Barris

et al. 2020

A&A

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AU Mic b is a Neptune-sized planet on an 8.47-day orbit around the nearest pre-main sequence (~20 Myr) star to the Sun, the bright (V = 8.81) M dwarf AU Mic. The planet was preliminary detected in Doppler radial velocity time series and recently confirmed to be transiting with data from the TESS mission. AU Mic b is likely to be cooling and contracting and might be accompanied by a second, more massive planet, in an outer orbit. Here, we present the observations of the transit of AU Mic b using ESPRESSO on the Very Large Telescope. We obtained a high-resolution time series of spectra to measure the Rossiter-McLaughlin effect, to constrain the spin-orbit alignment of the star and planet, and to simultaneously attempt to retrieve the planet’s atmospheric transmission spectrum. These observations allowed us to study, for the first time, the early phases of the dynamical evolution of young systems. We applied different methodologies to derive the spin-orbit angle of AU Mic b, and all of them retrieve values consistent with the planet being aligned with the rotation plane of the star. We determined a conservative spin-orbit angle λ value of −2.96−10.30+10.44 degrees, indicative that the formation and migration of the planets of the AU Mic system occurred within the disc. Unfortunately, and despite the large signal-to-noise ratio of our measurements, the degree of stellar activity prevented us from detecting any features from the planetary atmosphere. In fact, our results suggest that transmission spectroscopy for recently formed planets around active young stars is going to remain very challenging, if at all possible, for the near future.

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Section: Discussionmentioning

confidence: 85%

Transmission spectroscopy and Rossiter-McLaughlin measurements of the young Neptune orbiting AU Mic

Πάλλη

Oshagh

Casasayas-Barris

et al. 2020

A&A

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“…(Albrecht et al 2012b), 9(Masuda 2015), 10(Lund et al 2014), 11(Béky et al 2014), 12(Winn et al 2010), 13 (Sanchis-Ojeda & Winn 2011), 14(Esposito et al 2017), 15(Mancini et al 2018), 16(Mancini et al 2015), 17 (Mohler-Fischer et al 2013, 18(Mann et al 2020), 19(Dai et al 2020), 20(Henry & Winn 2008), 21(Cegla et al 2016), 22 (Maxted et al 2015, 23(Santos et al 2020), 24(Stefansson et al 2020), 25(Santerne et al 2016), 26(Hjorth et al 2019), 27(Hjorth et al 2021), 28(Wyttenbach et al 2020), 29(Ahlers et al 2020), 30(Zhou et al 2016), 31(Wang et al 2018), 32(Howarth & Morello 2017), 33(Désert et al 2011), 34 (McQuillan et al 2013, 35(Albrecht et al 2013), 36 (Sanchis-Ojeda et al 2013, 37(Johnson et al 2017), 38(Dorval et al 2020), 39(Mislis et al 2015), 40(Covino et al 2013), 41(Dai et al 2017), 42(Bryan et al 2012), 43(Močnik et al 2017), 44(Hirano et al 2020b), 45 (Sanchis-Ojeda et al 2011), 46 (Triaud et al 2010, 47(Gillon et al 2009), 48 (Tregloan-Reed et al 2015, 49(Albrecht et al 2012a), 50(Bourrier et al 2017), 51 (Tregloan-Reed et al 2013, 52(Brothwell et al 2014), 53(Brown et al 2012), 54(Johnson et al 2015), 55(Southworth et al 2016), 56…”

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A Preponderance of Perpendicular Planets

Albrecht,

Marcussen,

Winn

et al. 2021

Preprint

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Observing the Rossiter-McLaughlin effect during a planetary transit allows the determination of the angle λ between the sky projections of the star's spin axis and the planet's orbital axis. Such observations have revealed a large population of well-aligned systems and a smaller population of misaligned systems, with values of λ ranging up to 180 • . For a subset of 57 systems, we can now go beyond the sky projection and determine the 3-d obliquity ψ by combining the Rossiter-McLaughlin data with constraints on the line-of-sight inclination of the spin axis. Here we show that the misaligned systems do not span the full range of obliquities; they show a preference for nearly-perpendicular orbits (ψ = 80 − 125 • ) that seems unlikely to be a statistical fluke. If confirmed by further observations, this pile-up of polar orbits is a clue about the unknown processes of obliquity excitation and evolution.

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“…The TESS Hunt for Young and Maturing Exoplanets (THYME) Survey seeks to identify planets transiting stars in nearby, young, coeval populations. We have validated three systems to date: DS Tuc A b (Newton et al 2019), HIP 67522 b (Rizzuto et al 2020), and HD 63433 b and c (Mann et al 2020). Our work complements the efforts of other groups to discover young exoplanets, such as the Cluster Difference Imaging Photometric Survey (CDIPS; Bouma et al 2019) and the PSF-based Approach to TESS High quality data Of Stellar clusters project (PATHOS; Nardiello et al 2019).…”

Section: Introductionmentioning

confidence: 72%

TESS Hunt for Young and Maturing Exoplanets (THYME) IV: Three small planets orbiting a 120 Myr-old star in the Pisces--Eridanus stream

Newton,

Mann,

Kraus

et al. 2021

Preprint

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Young exoplanets can offer insight into the evolution of planetary atmospheres, compositions, and architectures. We present the discovery of the young planetary system TOI 451 (TIC 257605131, Gaia DR2 4844691297067063424). TOI 451 is a member of the 120-Myr-old Pisces-Eridanus stream (Psc-Eri). We confirm membership in the stream with its kinematics, its lithium abundance, and the rotation and UV excesses of both TOI 451 and its wide binary companion, TOI 451 B (itself likely an M dwarf binary). We identified three candidate planets transiting in the TESS data and followed up the signals with photometry from Spitzer and ground-based telescopes. The system comprises three validated planets at periods of 1.9, 9.2 and 16 days, with radii of 1.9, 3.1, and 4.1 R ⊕ , respectively. The host star is near-solar mass with V = 11.0 and H = 9.3 and displays an infrared excess indicative of a debris disk. The planets offer excellent prospects for transmission spectroscopy with HST and JWST, providing the opportunity to study planetary atmospheres that may still be in the process of evolving.

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TESS Hunt for Young and Maturing Exoplanets (THYME) III: a two-planet system in the 400 Myr Ursa Major Group

Cited by 10 publications

References 119 publications

Transmission spectroscopy and Rossiter-McLaughlin measurements of the young Neptune orbiting AU Mic

Transmission spectroscopy and Rossiter-McLaughlin measurements of the young Neptune orbiting AU Mic

A Preponderance of Perpendicular Planets

TESS Hunt for Young and Maturing Exoplanets (THYME) IV: Three small planets orbiting a 120 Myr-old star in the Pisces--Eridanus stream

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